On the "Lensing is Low" of BOSS Galaxies

Zu, Ying

doi:10.48550/arxiv.2010.01143

Cited by 14 publications

(19 citation statements)

References 82 publications

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“…Recently, Zu (2020) claimed that the lensing-is-low tension can be solved on small scales for both the CMASS sample analysed in Leauthaud et al (2017) and Yuan et al (2020b) and a LOWZ sub-sample very similar to the one studied in this work. The author can fit the large-scale clustering and lensing on small scales by predicting a large fraction of satellites in both galaxies samples.…”

Section: Lensing Is Lowmentioning

confidence: 58%

On the halo-mass and radial scale dependence of the lensing is low effect

Lange,

Leauthaud,

Singh

et al. 2020

Preprint

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The canonical ΛCDM cosmological model makes precise predictions for the clustering and lensing properties of galaxies. It has been shown that the lensing amplitude of galaxies in the Baryon Oscillation Spectroscopic Survey (BOSS) is lower than expected given their clustering properties. We present new measurements and modelling of galaxies in the BOSS LOWZ sample. We focus on the radial and stellar mass dependence of the lensing amplitude mis-match. We find an amplitude mismatch of around 35% when assuming ΛCDM with Planck Cosmological Microwave Background (CMB) constraints. This offset is independent of halo mass and radial scale in the range M halo ∼ 10 13.3 − 10 13.9 h −1 M and r = 0.1 − 60 h −1 Mpc (0.05 h/Mpc k 20 h/Mpc). The observation that the offset is both mass and scale independent places important constraints on the degree to which astrophysical processes (baryonic effects, assembly bias) can fully explain the effect. This scale independence also suggests that the "lensing is low" effect on small and large radial scales probably have the same physical origin. Resolutions based on new physics require a nearly uniform suppression, relative to ΛCDM predictions, of the amplitude of matter fluctuations on these scales. The possible causes of this are tightly constrained by measurements of the CMB and of the low-redshift expansion history.

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Section: Lensing Is Lowmentioning

confidence: 58%

On the halo-mass and radial scale dependence of the lensing is low effect

Lange,

Leauthaud,

Singh

et al. 2020

Preprint

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“…Recent work has shown that modifying the standard HOD formalism to include assembly bias does reduce the "lensing is low" discrepancy (e.g. Yuan et al 2021;Lange et al 2021;Zu 2020). The ability of relatively computationally efficient physics-based models, such as SAMs, to qualitatively reproduce the assembly bias signal seen in more sophisticated numerical hydrodynamic simulations is very promising for developing techniques to create large volume mock galaxy catalogs that are consistent with both lensing and galaxy clustering as well as other cosmological probes.…”

Section: Discussionmentioning

confidence: 99%

Galaxy assembly bias and large-scale distribution: a comparison between IllustrisTNG and a semi-analytic model

Hadzhiyska,

Liu,

Somerville

et al. 2021

Preprint

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In this work, we compare large scale structure observables for stellar mass selected samples at 𝑧 = 0, as predicted by two galaxy models, the hydrodynamical simulation IllustrisTNG and the Santa-Cruz semi-analytic model (SC-SAM). Although both models have been independently calibrated to match observations, rather than each other, we find good agreement between the two models for two-point clustering and galaxy assembly bias signatures. The models also show a qualitatively similar response of occupancy and clustering to secondary halo paramaters other than mass, such as formation history and concentration, although with some quantitative differences. Thus, our results demonstrate that the galaxy-halo relationships in SC-SAM and TNG are quite similar to first order. However, we also find areas in which the models differ. For example, we note a strong correlation between halo gas content and environment in TNG, which is lacking in the SC-SAM, as well as differences in the occupancy predictions for low-mass haloes. Moreover, we show that higher-order statistics, such as cumulants of the density field, help to accurately describe the galaxy distribution and discriminate between models that show degenerate behavior for two-point statistics. Our results suggest that SAMs are a promising cost-effective and intuitive method for generating mock catalogues for next generation cosmological surveys.

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“…We find the best-fitting values to be {lg 𝑀 ℎ =13.19, 𝑐=5.1, 𝑏=1.15, 𝜅=0.63, 𝛼=1.2}, and the best-fitting predictions of the total (blue solid) and resolved (red solid) signals are shown in the left main panel of Figure 5. The bias value is slightly higher than predicted for haloes with lg 𝑀 ℎ =13.19, primarily because a good fraction of the LRGs are satellite galaxies inside massive haloes (Zu 2020). Both predictions are in excellent agreement with the measurements, as demonstrated by the ratios between data and predictions in the left bottom panel of Figure 5.…”

Section: Reconstruct 3d Galaxy-cloud Cross-correlationmentioning

confidence: 61%

Kinematics of MgII Absorbers from the Redshift-space Distortion Around Massive Quiescent Galaxies

2021

Preprint

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The kinematics of MgII absorbers is the key to understanding the origin of cool, metalenriched gas clouds in the circumgalactic medium of massive quiescent galaxies. Exploiting the fact that the cloud line-of-sight velocity distribution is the only unknown for predicting the redshift-space distortion (RSD) of MgII absorbers from their 3D real-space distribution around galaxies, we develop a novel method to infer the cool cloud kinematics from the redshift-space galaxy-cloud cross-correlation 𝜉 𝑠 . We measure 𝜉 𝑠 for ∼10 4 MgII absorbers around ∼8×10 5 CMASS galaxies at 0.4<𝑧<0.8. We discover that 𝜉 𝑠 does not exhibit a strong Fingers-of-God effect, but is heavily truncated at velocity ∼300 km 𝑠 −1 . We reconstruct both the redshift and real-space cloud number density distributions inside haloes, 𝜉 𝑠 1ℎ and 𝜉 1ℎ , respectively. Thus, for any model of cloud kinematics, we can predict 𝜉 𝑠 1ℎ from the reconstructed 𝜉 1ℎ , and self-consistently compare to the observed 𝜉 𝑠 1ℎ . We consider four types of cloud kinematics, including an isothermal model with a single velocity dispersion, a satellite infall model in which cool clouds reside in the subhaloes, a cloud accretion model in which clouds follow the cosmic gas accretion, and a tired wind model in which clouds originate from the galactic wind-driven bubbles. All the four models provide statistically good fits to the RSD data, but only the tired wind model can reproduce the observed truncation by propagating ancient wind bubbles at ∼250 km 𝑠 −1 on scales ∼400 ℎ −1 kpc. Our method provides an exciting path to decoding the dynamical origin of metal absorbers from the RSD measurements with upcoming spectroscopic surveys.

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On the "Lensing is Low" of BOSS Galaxies

Cited by 14 publications

References 82 publications

On the halo-mass and radial scale dependence of the lensing is low effect

On the halo-mass and radial scale dependence of the lensing is low effect

Galaxy assembly bias and large-scale distribution: a comparison between IllustrisTNG and a semi-analytic model

Kinematics of MgII Absorbers from the Redshift-space Distortion Around Massive Quiescent Galaxies

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